The nature of bipolar outflows and the fates of stellar cluster-forming regions

Details The nature of bipolar outflows and the fates of stellar cluster-forming regions The nature of bipolar outflows and the fates of stellar cluster-forming regions

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19513507m&link_type=abstract

American Astronomical Society, 195th AAS Meeting, #135.07; Bulletin of the American Astronomical Society, Vol. 32, p.883

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We model the structure of protostellar winds and the dynamics of the molecular outflows they drive, and consider the implications of these outflows for the efficiency and dynamical evolution of dense regions in which star clusters are formed. We show that hydromagnetic winds from accreting protostars will assume a common force distribution at large distances, whether or not the wind emanates from a narrow region of disk radii. In any power-law density distribution, such a wind sweeps ambient gas into thin shells whose features match those commonly observed in bipolar molecular outflows, regardless how the driving wind's intensity varies over time. This implies that prompt entrainment, not turbulence, is responsible for these features. This model predicts the rate of mass ejection from a star-forming region, and thus the efficiency with which a star cluster can form. Using the energy injection and mass ejection implied by this model, we address the dynamical evolution of a dense clump inside a molecular cloud as it creates a cluster of low-mass stars. We use the virial equation of motion and assume that star formation is limited by ambipolar diffusion. For lower pressures than within starburst nuclei, an equilibrium state is possible if turbulence does not decay extremely rapidly. However, clumps tend to oscillate about their equilibria, and this can cause star formation to proceed in bursts.

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